2019A&A...624A.123P


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.18CEST06:15:08

2019A&A...624A.123P - Astronomy and Astrophysics, volume 624A, 123-123 (2019/4-1)

Gliese 49: activity evolution and detection of a super-Earth. A HADES and CARMENES collaboration.

PERGER M., SCANDARIATO G., RIBAS I., MORALES J.C., AFFER L., AZZARO M., AMADO P.J., ANGLADA-ESCUDE G., BAROCH D., BARRADO D., BAUER F.F., BEJAR V.J.S., CABALLERO J.A., CORTES-CONTRERAS M., DAMASSO M., DREIZLER S., GONZALEZ-CUESTA L., GONZALEZ HERNANDEZ J.I., GUENTHER E.W., HENNING T., HERRERO E., JEFFERS S.V., KAMINSKI A., KURSTER M., LAFARGA M., LETO G., LOPEZ-GONZALEZ M.J., MALDONADO J., MICELA G., MONTES D., PINAMONTI M., QUIRRENBACH A., REBOLO R., REINERS A., RODRIGUEZ E., RODRIGUEZ-LOPEZ C., SCHMITT J.H.M.M., SOZZETTI A., SUAREZ MASCARENO A., TOLEDO-PADRON B., ZANMAR SANCHEZ R., ZAPATERO OSORIO M.R. and ZECHMEISTER M.

Abstract (from CDS):


Context. Small planets around low-mass stars often show orbital periods in a range that corresponds to the temperate zones of their host stars which are therefore of prime interest for planet searches. Surface phenomena such as spots and faculae create periodic signals in radial velocities and in observational activity tracers in the same range, so they can mimic or hide true planetary signals.
Aims. We aim to detect Doppler signals corresponding to planetary companions, determine their most probable orbital configurations, and understand the stellar activity and its impact on different datasets.
Methods. We analyzed 22yr of data of the M1.5 V-type star Gl 49 (BD+61 195) including HARPS-N and CARMENES spectrographs, complemented by APT2 and SNO photometry. Activity indices are calculated from the observed spectra, and all datasets are analyzed with periodograms and noise models. We investigated how the variation of stellar activity imprints on our datasets. We further tested the origin of the signals and investigate phase shifts between the different sets. To search for the best-fit model we maximize the likelihood function in a Markov chain Monte Carlo approach.
Results. As a result of this study, we are able to detect the super-Earth Gl 49b with a minimum mass of 5.6M. It orbits its host star with a period of 13.85d at a semi-major axis of 0.090au and we calculate an equilibrium temperature of 350K and a transit probability of 2.0%. The contribution from the spot-dominated host star to the different datasets is complex, and includes signals from the stellar rotation at 18.86d, evolutionary timescales of activity phenomena at 40-80d, and a long-term variation of at least four years.

Abstract Copyright: © ESO 2019

Journal keyword(s): planetary systems - techniques: radial velocities - stars: late-type - stars: activity - stars: individual: Gl 49 - methods: data analysis

VizieR on-line data: <Available at CDS (J/A+A/624/A123): tablea1.dat>

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 BD+61 195 PM* 01 02 38.8679928575 +62 20 42.172837073   11.439   8.7   M1.5V 208 0
2 BD+61 195b Pl 01 02 38.8679928575 +62 20 42.172837073           ~ 3 0
3 2RXS J010318.3+622140 X 01 03 18.40 +62 21 40.8           ~ 1 0
4 Wolf 47 Er* 01 03 19.8342607685 +62 21 55.831198996   15.34 13.21 12.4   M5V 170 0
5 GJ 3942 PM* 16 09 03.1411378130 +52 56 37.958424161       9.706   M0.5Ve 50 0
6 NAME Barnard's star BY* 17 57 48.4997994034 +04 41 36.111354228 12.497 11.24 9.511 8.298 6.741 M4V 688 2

    Equat.    Gal    SGal    Ecl

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2021.05.18-06:15:08

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